I will present the current results of my on-going efforts to
accurately model the accretion streams in the magnetic
cataclysmic variable stars known as POLARS. I have developed
a computational code which uses SPH as a basis for tackling
the extrememly complex physics involved in the accretion
stream. The current version of the computational models
include an improved treatment of the motion along the
magnetically confined portion of the accretion stream which
allows the extraction of synthetic radial velocity data and
phase information for stream eclipses. I am currently
developing a secondary analysis code which will
automatically extract radial velocity data positions along
the entire stream from any specified inclination and phase.
The progress and initial results of the extraction code and
observational comparisons at the time of the conference will
be presented.

This work was supported by NASA/OSS NNG04GD62G NASA/MU-SPIN
NNG04GC40A, NASA/URC NCCW-0085 and NASA/PAIR NCC5-454

The author(s) of this abstract have provided an email address
for comments about the abstract:
jcash@physics.scsu.edu